From the Big Bang to Dark Energy Outline power spectrum
From the Big Bang to Dark Energy Hitoshi Murayama Kavli IPMU, University of Tokyo UC Berkeley, Lawrence Berkeley Laboratory
1 Credit:(NASA(
How did the Universe begin? What is its fate? What is it made of? What are its fundamental laws? Where do we come from? Now in the realm of science!
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2
Outline 1. From daily life to the Big Bang 2. Birth of elements and Higgs boson 3. Dark matter and anti-matter 4. Inflation and Dark energy
3
power spectrum
Credit: NASA
4
CMB protons
• photon pressure ⇒ “sound waves”
quasars
electrons
galaxies
cosmic microwave background recombina7on
•
before recombination, there was a fluid of protons, electrons, photons, dark matter (and neutrinos)
Big Bang
380k yrs
a few 100M yrs
13.8B yrs
7me
5 WMAP Wilkerson Microwave Anisotropy Probe
assump@on
Credit: NASA
• a random density
• “knows” about everything between 030% in the vicinity of the third acoustic peak (at l ≈ 800), while the two bins from l = 1000 to 1200 are new with the seven-year data analysis.
2.4. Temperature–Polarization (TE, TB) Cross Spectra The seven-year temperature–polarization cross-power spectra were formed using the same methodology as the five-year spectrum (Page et al. 2007; Nolta et al. 2009). For l ! 23, the cosmological model likelihood is estimated directly Credit: Wayne Hu from low-resolution temperature and polarization maps. The hLp://background.uchicago.edu/~whu/metaanim.html temperature input is a template-cleaned, co-added V + W-band map, while the polarization input is a template-cleaned, coadded Ka + Q + V-band map (Gold et al. 2009). In this regime, the spectrum can be inferred from the conditional likelihood of Cl values (individual or binned), but these estimates are only used for visualization. For l > 23, the temperature-polarization spectra are derived using the MASTER quadratic estimator, extended to include polarization data (Page et al. 2007). (As above, the MASTER spectrum is evaluated from l = 2, but the result from l = 2–23 is discarded.) The temperature input is a template-cleaned, co-added V+W-band map, while the polarization input is a template-cleaned, co-added Q+V+W-band map. The inclusion of W-band data in the high-l TE and TB spectra is new with the
7
spa@al curvature
4
Credit: NASA
Ωk changes the apparent angular size of the peak posi7ons
8
spa@al curvature
Credit: NASA
Credit: Wayne Hu hNp://background.uchicago.edu/~whu/animbut/anim3.html
Ωk changes the apparent angular size of the peak posi7ons
8
atoms
Credit: Wayne Hu hNp://background.uchicago.edu/~whu/animbut/anim1.html Credit: Wayne Hu hNp://background.uchicago.edu/~whu/animbut/anim1.html
Ωb changes the rela7ve size of even and odd peaks
9
atoms
Credit: Wayne Hu hNp://background.uchicago.edu/~whu/animbut/anim1.html Credit: Wayne Hu hNp://background.uchicago.edu/~whu/animbut/anim1.html
Ωb changes the rela7ve size of even and odd peaks
9
Credit: NASA
Energy Budget of the Universe
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5%
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5% • Neutrinos are ~0.1–0.7%
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5% • Neutrinos are ~0.1–0.7% • Rest of ordinary matter
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
(electrons, protons & neutrons) are ~4.4%
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5% • Neutrinos are ~0.1–0.7% • Rest of ordinary matter
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
(electrons, protons & neutrons) are ~4.4%
• Dark Matter ~25%
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5% • Neutrinos are ~0.1–0.7% • Rest of ordinary matter • •
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
(electrons, protons & neutrons) are ~4.4% Dark Matter ~25% Dark Energy ~70%
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5% • Neutrinos are ~0.1–0.7% • Rest of ordinary matter
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
(electrons, protons & neutrons) are ~4.4% Dark Matter ~25% Dark Energy ~70%
• • • Anti-Matter 0%
10
3. Dark maLer and an@-‐maLer
11
dark maLer
12
solar system
Credit: NASA/JPL
13
solar system
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
13
solar system
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
13
1 v/p r
solar system
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
13
a hundred billion stars
28,000 lyrs
Credit: NASA
14 solar system revolves at 220 km/s what is pulling us inside?
a hundred billion stars
28,000 lyrs
Credit: NASA
14 solar system revolves at 220 km/s what is pulling us inside?
a hundred billion stars
28,000 lyrs
Credit: NASA
14 solar system revolves at 220 km/s what is pulling us inside?
a hundred billion stars
28,000 lyrs no stars
Credit: NASA
14
Credit: Jschulman555 hLp://commons.wikimedia.org/wiki/File:NGC_4565_and_4562.jpg
15
Andromeda=2.5M lyrs away also dark maNer important
Credit: NASA
16
Credit: ESA/Hubble and NASA
17
Credit: Vicent Peris, CC BY-‐SA 2.0 hLp://commons.wikimedia.org/wiki/File:NGC_7331_-‐_Peris.jpg
18
Credit: Vicent Peris, CC BY-‐SA 2.0 hLp://commons.wikimedia.org/wiki/File:NGC_7331_-‐_Peris.jpg
18
Vera Rubin 1970’s
Credit: NOAO/AURA/NSF
19
true nature of galaxies 100k lyrs stars
dark maLer
>M lyrs
20
Credit: Based on observa7ons made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collabora7on between the Space Telescope Science Ins7tute (STScI/NASA), the Space Telescope European Coordina7ng Facility (ST-‐ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA), Image processed by c_cld hNp:// www.galaxyzooforum.org/index.php?topic=6927.msg610555#msg610555
21
Credit: Based on observa7ons made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collabora7on between the Space Telescope Science Ins7tute (STScI/NASA), the Space Telescope European Coordina7ng Facility (ST-‐ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA), Image processed by c_cld hNp:// www.galaxyzooforum.org/index.php?topic=6927.msg610555#msg610555
Cheshire cat
21
cluster of galaxies
Abell 2218 2.1B lyrs Credit: Andrew Fruchter (STScI) et al., WFPC2, HST, NASA
22
Credit: NASA, ESA & L. Calçada
deflec@on angle by a point lens ✓=
4GN m c 2 rc
23
Credit: NASA, ESA & L. Calçada
deflec@on angle by a point lens ✓=
Credit: NASA, Andrew Fruchter and the ERO Team [Sylvia BaggeL (STScI), Richard Hook (ST-‐ECF), Zoltan Levay (STScI)] (STScI)
4GN m c 2 rc
23
Credit: NASA, ESA & L. Calçada
deflec@on angle by a point lens ✓=
Credit: NASA, Andrew Fruchter and the ERO Team [Sylvia BaggeL (STScI), Richard Hook (ST-‐ECF), Zoltan Levay (STScI)] (STScI)
4GN m c 2 rc Credit: J. A. Tyson, UC Davis, LSST
23
image invisible dark maNer
more than 80% of maLer in the Universe is not atoms
24
image invisible dark maNer
more than 80% of maLer in the Universe is not atoms
24
image invisible dark maNer
more than 80% of maLer in the Universe is not atoms
24
4B lyrs away
25
Good not to be here
4B lyrs away
25
Good not to be here
two clusters collided at 4500km/sec 4B lyrs away
25
Good not to be here
two clusters collided at 4500km/sec Credit: J. Wise, M. Bradac (Stanford, KIPAC)
4B lyrs away
25
Good not to be here
two clusters collided at 4500km/sec Credit: J. Wise, M. Bradac (Stanford, KIPAC)
4B lyrs away
25
Good not to be here bullet cluster
two clusters collided at 4500km/sec Credit: J. Wise, M. Bradac (Stanford, KIPAC)
4B lyrs away
25
rs ly 2B
2B lyrs
nearly uniform small wrinkles
rs ly 2B Credit: Sloan Digital Sky Survey
26
10–5 Credit: NASA
we wouldn’t exist without dark maNer
without dark maLer
with dark maLer
27
Reenac@ng the Big Bang with Cal Marching Band
Nobelist George Smoot Directs Big Bang with Cal Band, 12/06 hLp://www.youtube.com/watch?v=OdsWhHWdc1g
28
Reenac@ng the Big Bang with Cal Marching Band
Credit: The Regents of the University of California Nobelist George Smoot Directs Big Bang with Cal Band, 12/06 hLp://www.youtube.com/watch?v=OdsWhHWdc1g
28
OK, I see dark maLer is important. What we do know about it? 29
Cold and Neutral •it must be moving slowly (cold) •it must be electrically neutral •it must be long-lived (at least 13.8Byrs)
30
Dim Stars? Search for MACHOs (Massive Compact Halo Objects) Large Magellanic Cloud
Credit: NASA
31
Dim Stars? Search for MACHOs (Massive Compact Halo Objects) Large Magellanic Cloud Credit: Hubble Heritage Team (AURA/STSCI/NASA)
Credit: NASA
31
Dim Stars? Search for MACHOs (Massive Compact Halo Objects) Large Magellanic Cloud Credit: Hubble Heritage Team (AURA/STSCI/NASA)
Credit: NASA
31
Dim Stars? Search for MACHOs (Massive Compact Halo Objects) Large Magellanic Cloud Credit: Hubble Heritage Team (AURA/STSCI/NASA)
Credit: NASA
Not enough of them!
31
Dim Stars? 0.6
Search for MACHOs (Massive Compact Halo Objects)
EROS collabora@on astro-‐ph/0607207 f = T−7
0.4
Large Magellanic Cloud
MACHO 95% cl EROS−2 + EROS−1 upper limit (95% cl)
0.2
Credit: Hubble Heritage Team 0.0 (AURA/STSCI/NASA) −8 −6 −4 −2
2 0 logM= 2log( t E /70d)
Credit: NASA
Not enough of them!
31
Mass Limits “Uncertainty Principle” •Clumps to form structure •imagine V = G Mrm •“Bohr radius”: r = G M m •too small m ⇒ won’t “fit” in a galaxy! •m >10 eV “uncertainty principle” N
2
B
N
2
−22
bound (modified from Hu, Barkana, Gruzinov, astro-ph/0003365)
32
Summary Mass Limits
Fritz Zwicky Credit: NASA/CXC/ SAO
33
Summary Mass Limits • 10
-31
GeV to 1050 GeV
Fritz Zwicky Credit: NASA/CXC/ SAO
33
Summary Mass Limits • 10 GeV to 10 GeV • narrowed it down to -31
50
within 81 orders of magnitude
Fritz Zwicky Credit: NASA/CXC/ SAO
33
Summary Mass Limits • 10 GeV to 10 GeV • narrowed it down to -31
50
within 81 orders of magnitude
• a big progress in 70 years since Zwicky
Fritz Zwicky Credit: NASA/CXC/ SAO
33
Self-‐Coupling
• if self-coupling too big, will •
“smooth out” cuspy profile at the galactic center some people want it (Spergel and Steinhardt, astro-ph/ 9909386)
• need core < 35 kpc/h from data σ < 1.7 x 10-25 cm2 (m/GeV)
(Yoshida, Springel, White, astro-ph/ 0006134)
• bullet cluster:
σ < 1.7x10-24 cm2 (m/GeV) (Markevitch et al, astro-ph/0309303)
34
•
Self-‐Coupling if self-coupling too big, will “smooth out” cuspy profile at the galactic center
• some people want it
(Spergel and Steinhardt, astro-ph/ 9909386)
• need core < 35 kpc/h from data σ < 1.7 x 10-25 cm2 (m/GeV)
(Yoshida, Springel, White, astro-ph/ 0006134)
• bullet cluster:
σ < 1.7x10-24 cm2 (m/GeV) (Markevitch et al, astro-ph/0309303)
Yoshida et al., 2000
34
MACHO ⇒ WIMP
Credit: NASA
35
MACHO ⇒ WIMP
Credit: NASA
35
MACHO ⇒ WIMP • It is probably WIMP (Weakly Interacting Massive Particle)
• Stable heavy particle produced in early Universe, left-over from near-complete annihilation
• Will focus on WIMPs for the rest or the lecture
Credit: NASA
35 G. Jungman et al. JPhysics Reports 267 (1996) 195-373
221
Using the above relations (H = 1.66g$‘2T 2/mpl and the freezeout condition r = Y~~(G~z~) = H), we find (n&)0 = (n&f
= 1001(m,m~~g~‘2+JA+)
N 10-S/[(m,/GeV)((~A~)/10-27
cm3 s-‘)I,
thermal relic
(3.3)
where the subscript f denotes the value at freezeout and the subscript 0 denotes the value today. The current entropy density is so N 4000 cmm3, and the critical density today is pC II 10-5h2 GeVcmp3, where h is the Hubble constant in units of 100 km s-l Mpc-‘, so the present mass density in units of the critical density is given by 0,h2 = mxn,/p, N (3 x 1O-27 cm3 C1/(oAv))
• • • • • •
.
(3.4)
The result is independent of the mass of the WIMP (except for logarithmic corrections), and is inversely proportional to its annihilation cross section. Fig. 4 shows numerical solutions to the Boltzmann equation. The equilibrium (solid line) and actual (dashed lines) abundances per comoving volume are plotted as a function of x = m,/T
thermal equilibrium when kT>mχc2 Once kT<mχc2, no more χ created if stable, only way to lose them is annihilation but universe expands and χ get dilute at some point they can’t find each other their number in comoving volume “frozen”
0 . 01 0 . 001
0 . 0001 10-b
10-s
,h -;
10-7
caJ 10-a
a
10-Q
2 p
lo-‘9
$
lo-”
z
10-m
F!
lo-‘3
10
x=m/T
100
(time
Fig. 4. Comoving number density of a WIMP in the early Universe. the solid curve is the equilibrium abundance. From [31].
+) The dashed
curves are the actual abundance,
and
36
Order of magnitude • “Known” Ω =0.23 χ
determines the WIMP annihilation cross section
• simple estimate of
⇤ g⇥
⌅⇤ann v⇧ ⇤
the annihilation cross ⇥ 10 section
• within the range at LHC!!!
1/2
xf s0 MP3 l ⌅⇤ann v⇧ H02
1.12
GeV 2 ⇥ 2 ⌅⇤ann v⇧ ⇤ 2 m m ⇤ 300 GeV 9
10
10
GeV
1/2 g⇥
2
xf
h2
37
Listen to faint sound can’t hear faint sound
38
Listen to faint sound can’t hear faint sound
shut out the noise!
38
Listen to faint sound can’t hear faint sound
shut out the noise!
to hear faint sound of dark maLer ???? go to quiet space＝underground
38
Listen to faint sound can’t hear faint sound
shut out the noise!
to hear faint sound of dark maLer go to quiet space＝underground
38
39
basic idea • maximum energy
nucleus
transfer to nucleus when mχ~MA
DM
nucleus
• energy of the nucleus leads to a combination of
• ionization • phonon • scintillation
DM
Ef =
1 m MA m v2 2(1 2 (m + MA )2
ˆ cos ✓)
40 December 24, 2009
2010 Jan 21
Y. Suzuki (IPMU Site Visit) @Kashiwa
25
41
XMASS 1t liquid Xenon in Kamioka mine
42 Rene Ong
WIMP Direct Detection Limits Spin Independent
Spin Dependent
potential signals
COUPP Xenon100
Super K Super-K
MSSM
IceCube
MSSM
(Potential signals: DAMA/LIBRA, CRESST, CoGeNT – see backup slides)
43 Rene Ong
WIMP Direct Detection Limits
Exci7ng! Spin Independent
Spin Dependent
potential signals
COUPP Xenon100
Super K Super-K
MSSM
IceCube
MSSM
(Potential signals: DAMA/LIBRA, CRESST, CoGeNT – see backup slides)
43
LHC E=mc2 Credit: CERN, Photograph: Maximilien Brice
Can we make dark maNer? Credit: CERN
44
• Something is escaping the detector ⇒Dark Matter!?
| 500cm
0
energy and momenta are unbalanced “missing energy” Emiss
Y
• Mimic Big Bang in the lab • Hope to create invisible Dark Matter particles • Look for events where
4.8Gev EC 19.Gev HC
500cm|
Producing Dark MaLer in the laboratory
| 500cm YX hist.of BA.+E.C.
0
X
500cm|
Credit: CERN
45
program
cosmic abundance
of dark matter • cosmological measurement −1 abundance ∝ σ • ann • detection experiments • scattering cross section • production at colliders • mass, couplings • can calculate cross sections • If they agree with each other:
⇒ ⇒
LHC
WMAP
Will know what Dark MaHer is Will understand universe back to t∼10-10 sec
ILC
mass of the Dark Matter
46
yrs
yrs
8B
0k
t ion rill
in
13.
38
3m
1t ec hs
CMB
Higgs
Credit: C. Amsler et al. (Par@cle Data Group), Physics LeLers B667, 1 (2008)
47
yrs
yrs
8B
0k
in
13.
38
3m
sec nth llio -bi ten sec th ion rill
1t
Higgs DM
CMB
Credit: C. Amsler et al. (Par@cle Data Group), Physics LeLers B667, 1 (2008)
47
Neutrinos and an@-‐maLer
48
Credit: NASA
49
Credit: NASA
49
An@-‐MaLer •for every particle, there is an antiparticle
•same mass, same lifetime •opposite electric charge •electron e and positron e_ •proton p and anti-proton p _ •neutron n and anti-neutron n –
+
50
51
1933 first humanmade an@-‐maLer
51
γ photon 1933 first humanmade an@-‐maLer
51
e− electron
γ photon 1933 first humanmade an@-‐maLer
51
e− electron
e+ positron
γ photon 1933 first humanmade an@-‐maLer
51
e− electron
Irène
e+ positron
γ photon Frédéric Joliot-‐Curie
1933 first humanmade an@-‐maLer
51
Berkeley
Credit: © 2010 The Regents of the University of California, Lawrence Berkeley Na@onal Laboratory
52
Berkeley
1955 an@-‐proton
maLer and an@-‐ maLer annihilate into pure energy Credit: © 2010 The Regents of the University of California, Lawrence Berkeley Na@onal Laboratory
52
Berkeley
1955 an@-‐proton
Emilio Owen Segrè Chamberlain maLer and an@-‐ maLer annihilate into pure energy Credit: © 2010 The Regents of the University of California, Lawrence Berkeley Na@onal Laboratory
Credit: CERN
\CM : $ &#IMP
8
CM\
'EV%# 'EV(#
Q
52
53
98HISTOF"! %# \CM
9
CM\
an@-‐maLer at use
Positron Emission Tomography (PET)
Typical PET Facility
54
Credit: NIDA, NIH
55
56
Credit: Positronics Research, LLC
56
Credit: Positronics Research, LLC
E=mc2 300 million @mes more efficient than regular gasoline
56
Energy sources •eV=1.6×10 J •for each proton m c =0.938GeV •chemical reaction ~eV •nuclear fission ~MeV •nuclear fusion ~10MeV •anti-matter (proton on anti-proton) –19
p
2
~GeV
57
58
• European Laboratory CERN
• A scientist produced
a quarter gram of anti-matter without the knowledge of the Director General
• falls into wrong hands!
58
• European Laboratory CERN
• A scientist produced
a quarter gram of anti-matter without the knowledge of the Director General
• falls into wrong hands!
billion trillion trillion dollars
58
• European Laboratory CERN
• A scientist produced
a quarter gram of anti-matter without the knowledge of the Director General
• falls into wrong hands!
billion trillion trillion dollars
58
Early Universe 1,000,000,002
1,000,000,000
matter
anti-matter 59
Current Universe 2 us
anti-matter
matter
We won! But why?
60
Beginning of Universe 1,000,000,001
1,000,000,001
anti-matter
matter
61
frac@on of second later 1 1,000,000,002
matter
1,000,000,000
anti-matter
turned a billionth of an@-‐maLer to maLer
62
Universe Now 2 us
matter
anti-matter
This must be how we survived the Big Bang!
63
Life or Death
64
Life or Death • Is the world of anti-matter the exact mirror of the world of matter?
64
Life or Death • Is the world of anti-matter the exact mirror of the world of matter? • If so, there is no reason for matter to be chosen
64
Life or Death • Is the world of anti-matter the exact mirror of the world of matter? • If so, there is no reason for matter to be chosen • It shouldn’t be an exact mirror. There must be some subtle difference!
64
Life or Death • Is the world of anti-matter the exact mirror of the world of matter? • If so, there is no reason for matter to be chosen • It shouldn’t be an exact mirror. There must be some subtle difference! • How can such a difference be explained? 64
Life or Death • Is the world of anti-matter the exact mirror of the world of matter? • If so, there is no reason for matter to be chosen • It shouldn’t be an exact mirror. There must be some subtle difference! • How can such a difference be explained? • A bold 1973 theory by Kobayashi and Maskawa (2008 Nobel prize in physics)
64
Elementary Par@cles Credit: Marekich, CC BY-‐SA 3.0
nuclei
atoms
protons
neutrons
quarks
Credit: NASA
65
Elementary Par@cles Credit: Marekich, CC BY-‐SA 3.0
nuclei
atoms
protons
neutrons
quarks down
Credit: NASA
up
65
Elementary Par@cles Credit: Marekich, CC BY-‐SA 3.0
nuclei
atoms
protons
neutrons
quarks down
Credit: NASA
electron
down
up
up
65
Elementary Par@cles Credit: Marekich, CC BY-‐SA 3.0
nuclei
atoms
protons
neutrons
quarks down
Credit: NASA
muon
electron
down
up
up
65
Elementary Par@cles Credit: Marekich, CC BY-‐SA 3.0
nuclei
atoms
protons Who ordered that?? muon I.I. Rabi electron down
neutrons
quarks down
Credit: NASA
up
up
65
Muons
66
Muons
Muons come from outer space. About a thousand of them go through our body every minute like X-‐ray.
66 Science 167, 832 (1970)
Credit: Ricardo Liberato, CC BY-‐SA 3.0
Search for Hidden Chambers in the Pyramids The structure of the Second Pyramid of Giza is determined by cosmic-ray absorption Luis W. Alvarez, Jared A. Anderson, F. El Bedwei, James Burkhard, Ahmed Fakhry, Adib Girgis, Amr Goneid, Fikhry Hassan, Dennis Iverson, Gerald Lynch, Zenab Miligy, Ali Hilmy Moussa, Mohammed Sharkawi, Lauren Yazolino
67 Science 167, 832 (1970)
Credit: Ricardo Liberato, CC BY-‐SA 3.0
Search for Hidden Chambers in the Pyramids The structure of the Second Pyramid of Giza is determined by cosmic-ray absorption Luis W. Alvarez, Jared A. Anderson, F. El Bedwei, James Burkhard, Ahmed Fakhry, Adib Girgis, Amr Goneid, Fikhry Hassan, Dennis Iverson, Gerald Lynch, Zenab Miligy, Ali Hilmy Moussa, Mohammed Sharkawi, Lauren Yazolino
67
Credit: Ricardo Liberato, CC BY-‐SA 3.0
Science 167, 832 (1970) Search for Hidden Chambers in the Pyramids The structure of the Second Pyramid of Giza is determined by cosmic-ray absorption Luis W. Alvarez, Jared A. Anderson, F. El Bedwei, James Burkhard, Ahmed Fakhry, Adib Girgis, Amr Goneid, Fikhry Hassan, Dennis Iverson, Gerald Lynch, Zenab Miligy, Ali Hilmy Moussa, Mohammed Sharkawi, Lauren Yazolino
hidden chamber with treasures?
67 Credit: Ricardo Liberato, CC BY-‐SA 3.0
Science 167, 832 (1970) Search for Hidden Chambers in the Pyramids The structure of the Second Pyramid of Giza is determined by cosmic-ray absorption Luis W. Alvarez, Jared A. Anderson, F. El Bedwei, James Burkhard, Ahmed Fakhry, Adib Girgis, Amr Goneid, Fikhry Hassan, Dennis Iverson, Gerald Lynch, Zenab Miligy, Ali Hilmy Moussa, Mohammed Sharkawi, Lauren Yazolino
hidden chamber with treasures?
67 Credit: Ricardo Liberato, CC BY-‐SA 3.0
Science 167, 832 (1970) Search for Hidden Chambers in the Pyramids The structure of the Second Pyramid of Giza is determined by cosmic-ray absorption Luis W. Alvarez, Jared A. Anderson, F. El Bedwei, James Burkhard, Ahmed Fakhry, Adib Girgis, Amr Goneid, Fikhry Hassan, Dennis Iverson, Gerald Lynch, Zenab Miligy, Ali Hilmy Moussa, Mohammed Sharkawi, Lauren Yazolino
hidden chamber with treasures?
No hidden chamber!
•
67
see through a volcano use cosmic ray muons to see the inside of a volcano
•can locate magma •demonstrated by
Earthquake Research Institute, Univ. of Tokyo
•useful for
predicting eruption
Credit: © Center for High Energy Geophysics Research, Earthquake Research Ins@tute, University of Tokyo
68
•
see through a volcano use cosmic ray muons to see the inside of a volcano
•can locate magma •demonstrated by
Earthquake Research Institute, Univ. of Tokyo
•useful for
predicting eruption
Credit: © Center for High Energy Geophysics Research, Earthquake Research Ins@tute, University of Tokyo
68
69 Luis Walter Alvarez
69
Elementary Par@cles
muon electron
down
up
70
Elementary Par@cles
muon
strange
electron
down
up
70
Elementary Par@cles
Credit: NIMSoffice, CC BY-‐SA 3.0
There must be three of each type muon
strange
electron
down
up
70
Elementary Par@cles
Credit: NIMSoffice, CC BY-‐SA 3.0
There must be three of each type muon
strange
electron
down
charm
1974
up
70
Elementary Par@cles
Credit: NIMSoffice, CC BY-‐SA 3.0
There must be tau of e1975 three ach type muon electron
strange down
charm
1974
up
70
Elementary Par@cles
Credit: NIMSoffice, CC BY-‐SA 3.0
There must be bottom tau of e1975 three ach type muon
1978
strange
electron
charm
down
1974
up
70
Elementary Par@cles top
1995
Credit: NIMSoffice, CC BY-‐SA 3.0
There must be bottom tau of e1975 three ach type muon electron
strange down
1978
charm
1974
up
70
Why three?
71
Why three? • essential difference
between two and three
71
Why three? • essential difference between two and three • connect the dots
71
Why three? • essential difference between two and three • connect the dots
71
Why three? • essential difference between two and three • connect the dots
71
Why three? • essential difference between two and three • connect the dots
71
Why three? • essential difference between two and three • connect the dots
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter
correspond to reflection
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter
correspond to reflection
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter correspond to reflection • can make a difference!
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter correspond to reflection • can make a difference!
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter correspond to reflection • can make a difference!
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter correspond to reflection • can make a difference!
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter correspond to reflection • can make a difference! • but with two dots, a polygon collapses
71
Major experiments
Credit: SLAC Na@onal Accelerator Laboratory
72
Major experiments
•Head-to-head competition between
Stanford/Berkeley and KEK (Japan)
Credit: SLAC Na@onal Accelerator Laboratory
72
Major experiments
•Head-to-head competition between
Stanford/Berkeley and KEK (Japan)
•
Credit: SLAC Na@onal Accelerator Laboratory
Super high-tech machine with micron precision over 4 miles and colliding beams every 4 nanoseconds at speed of light
72
Credit: © 2009 The Regents of the University of California
73
Credit: © 2009 The Regents of the University of California
73
Difference between maLer and an@-‐maLer
74
Difference between maLer and an@-‐maLer
• Three found as they predicted
74
Difference between maLer and an@-‐maLer
• Three found as they predicted
• Then there must be
some difference between matter and anti-matter!
74
Difference between maLer and an@-‐maLer
• Three found as they predicted
• Then there must be
some difference between matter and anti-matter!
• Experiments at
Stanford and KEK confirmed their prediction precisely since 2002
74
• Three found as they predicted
• Then there must be
some difference between matter and anti-matter!
• Experiments at
Stanford and KEK confirmed their prediction precisely since 2002
Asymmetry Entries / 0.5 ps
Difference between maLer and an@-‐maLer
Belle
0
0
400 (d) B m J/YK 300 200 B0 100 0
_ B0
q=+1 q= 1
0.5 0
-0.5 -7.5 -5 -2.5
0
2.5
-X f $t(ps)
5
7.5
74
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
75
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
•We could explain the subtle difference
between matter and anti-matter thanks to Kobayashi and Maskawa
75
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
•We could explain the subtle difference •
between matter and anti-matter thanks to Kobayashi and Maskawa Can we then explain the difference of one part in billion in our Universe?
75
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
•We could explain the subtle difference • •
between matter and anti-matter thanks to Kobayashi and Maskawa Can we then explain the difference of one part in billion in our Universe? We can only explain 10–26!
75
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
•We could explain the subtle difference • • •
between matter and anti-matter thanks to Kobayashi and Maskawa Can we then explain the difference of one part in billion in our Universe? We can only explain 10–26! more differences are needed
75
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
•We could explain the subtle difference • • • •
between matter and anti-matter thanks to Kobayashi and Maskawa Can we then explain the difference of one part in billion in our Universe? We can only explain 10–26! more differences are needed we also need to see how anti-matter can turn into matter
75
New Paradigm •Maybe neutrinos could reshuffle the
balance between matter and anti-matter
•Possible if neutrino can morph into antineutrino and back
•Then we owe our existence to neutrinos!
76
New Paradigm •Maybe neutrinos could reshuffle the
balance between matter and anti-matter
•Possible if neutrino can morph into antineutrino and back
•Then we owe our existence to neutrinos! Fukugita Yanagida
76
Neutrinos morph KamLAND
1kt
uses mineral oil (liquid scin@llator) instead of water
Credit: KamLAND collabora@on
77
78
• • •
Credit: KamLAND collabora@on
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2
Survival Probability
Neutrinos morph There are three types of neutrinos (electron, muon, tau) one species changes into another neutrinos oscillate
1 0.8 ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.6 0.4 0.2 0 10
-3
10
-2
10
-1
10
1
20
30
40
50
60
70
80
L 0/E (km/MeV)
79
Neutrinos morph
• There are three types of neutrinos (electron, muon, tau) • one species changes into another • neutrinos oscillate
1 0.8 ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.6 0.4
0 10
-3
10
-2
10
h
0.2
p mor
Survival Probability
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2
Credit: KamLAND collabora@on
-1
10
1
20
30
40
50
60
70
80
L 0/E (km/MeV)
79
Neutrinos morph
• There are three types of neutrinos (electron, muon, tau) • one species changes into another • neutrinos oscillate
1 0.8
0.2 0 10
-3
10
-2
10
-1
ba ck
0.4
h
ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.6
p mor
Survival Probability
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2
Credit: KamLAND collabora@on
1
10
20
30
40
50
60
70
80
L 0/E (km/MeV)
79
Neutrinos morph
• There are three types of neutrinos (electron, muon, tau) • one species changes into another • neutrinos oscillate
1 0.8 ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.4
0 10
-3
10
-2
10
h
0.2
m or ph
ba ck
0.6
p mor
Survival Probability
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2
Credit: KamLAND collabora@on
-1
10
1
20
30
40
50
60
70
80
L 0/E (km/MeV)
79
• • •
Credit: KamLAND collabora@on
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2 1
0 10
-3
10
-2
10
ck
h
0.2
m or ph
ba
0.4
-1
10
1
20
30
40
ba
ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.6
ck
0.8
p mor
Survival Probability
Neutrinos morph There are three types of neutrinos (electron, muon, tau) one species changes into another neutrinos oscillate
50
60
70
80
L 0/E (km/MeV)
79
Neutrinos morph
• There are three types of neutrinos (electron, muon, tau) • one species changes into another • neutrinos oscillate
1
0.2 0 10
-3
10
-2
10
-1
m or ph
ba ck
0.4
h
ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.6
1
10
20
30
40
ba ck
0.8
p mor
Survival Probability
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2
Credit: KamLAND collabora@on
50
60
70
80
L 0/E (km/MeV)
79
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
80
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
80
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
80
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
80
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
80
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
paLence!
80
Need big underground experiments • look for 136 Xe ! 136 Ba e • dissolve gaseous xenon
e
into liquid scintillator
• current 100kg of enriched xenon
• so far only upper25limit
⌧1/2 > 3.4 ⇥ 10 years
KamLAND=1000t
Credit: KamLAND collabora@on
81
Need big underground experiments • look for 136 Xe ! 136 Ba e • dissolve gaseous xenon
e
into liquid scintillator
• current 100kg of enriched xenon
• so far only upper25limit
⌧1/2 > 3.4 ⇥ 10 years
KamLAND=1000t
Credit: KamLAND collabora@on
81
look for difference _ between ν and ν T2K
compare P (⌫µ ! ⌫e ) and P (¯⌫µ ! ⌫¯e )
82
1300km!
83
yrs
rs
ky
8B
13.
380
in 3m
ec th s lion -bil sec ten nth illio
1 tr
Higgs
CMB
DM
Credit: C. Amsler et al. (Par@cle Data Group), Physics LeLers B667, 1 (2008)
84
8B
13. yrs
rs
ky
DM
380
10
in 3m
ec th s lion -bil sec ten nth illio nds eco -26 s 1 tr
Higgs an7-‐maNer!
CMB
Credit: C. Amsler et al. (Par@cle Data Group), Physics LeLers B667, 1 (2008)
84
1 Credit:(NASA(
How did the Universe begin? What is its fate? What is it made of? What are its fundamental laws? Where do we come from? Now in the realm of science!
Credit:(aNGeLic!(by(Rolfe(Kolbe( CC BY 2.0 h7p://www.flickr.com/photos/46210293@N08/8287418426/(
2
Outline 1. From daily life to the Big Bang 2. Birth of elements and Higgs boson 3. Dark matter and anti-matter 4. Inflation and Dark energy
3
power spectrum
Credit: NASA
4
CMB protons
• photon pressure ⇒ “sound waves”
quasars
electrons
galaxies
cosmic microwave background recombina7on
•
before recombination, there was a fluid of protons, electrons, photons, dark matter (and neutrinos)
Big Bang
380k yrs
a few 100M yrs
13.8B yrs
7me
5 WMAP Wilkerson Microwave Anisotropy Probe
assump@on
Credit: NASA
• a random density
• “knows” about everything between 030% in the vicinity of the third acoustic peak (at l ≈ 800), while the two bins from l = 1000 to 1200 are new with the seven-year data analysis.
2.4. Temperature–Polarization (TE, TB) Cross Spectra The seven-year temperature–polarization cross-power spectra were formed using the same methodology as the five-year spectrum (Page et al. 2007; Nolta et al. 2009). For l ! 23, the cosmological model likelihood is estimated directly Credit: Wayne Hu from low-resolution temperature and polarization maps. The hLp://background.uchicago.edu/~whu/metaanim.html temperature input is a template-cleaned, co-added V + W-band map, while the polarization input is a template-cleaned, coadded Ka + Q + V-band map (Gold et al. 2009). In this regime, the spectrum can be inferred from the conditional likelihood of Cl values (individual or binned), but these estimates are only used for visualization. For l > 23, the temperature-polarization spectra are derived using the MASTER quadratic estimator, extended to include polarization data (Page et al. 2007). (As above, the MASTER spectrum is evaluated from l = 2, but the result from l = 2–23 is discarded.) The temperature input is a template-cleaned, co-added V+W-band map, while the polarization input is a template-cleaned, co-added Q+V+W-band map. The inclusion of W-band data in the high-l TE and TB spectra is new with the
7
spa@al curvature
4
Credit: NASA
Ωk changes the apparent angular size of the peak posi7ons
8
spa@al curvature
Credit: NASA
Credit: Wayne Hu hNp://background.uchicago.edu/~whu/animbut/anim3.html
Ωk changes the apparent angular size of the peak posi7ons
8
atoms
Credit: Wayne Hu hNp://background.uchicago.edu/~whu/animbut/anim1.html Credit: Wayne Hu hNp://background.uchicago.edu/~whu/animbut/anim1.html
Ωb changes the rela7ve size of even and odd peaks
9
atoms
Credit: Wayne Hu hNp://background.uchicago.edu/~whu/animbut/anim1.html Credit: Wayne Hu hNp://background.uchicago.edu/~whu/animbut/anim1.html
Ωb changes the rela7ve size of even and odd peaks
9
Credit: NASA
Energy Budget of the Universe
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5%
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5% • Neutrinos are ~0.1–0.7%
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5% • Neutrinos are ~0.1–0.7% • Rest of ordinary matter
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
(electrons, protons & neutrons) are ~4.4%
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5% • Neutrinos are ~0.1–0.7% • Rest of ordinary matter
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
(electrons, protons & neutrons) are ~4.4%
• Dark Matter ~25%
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5% • Neutrinos are ~0.1–0.7% • Rest of ordinary matter • •
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
(electrons, protons & neutrons) are ~4.4% Dark Matter ~25% Dark Energy ~70%
10
Credit: NASA
Energy Budget of the Universe
• Stars and galaxies are only ~0.5% • Neutrinos are ~0.1–0.7% • Rest of ordinary matter
Credit: NASA
Planck stars neutrinos baryon dark maNer dark energy
(electrons, protons & neutrons) are ~4.4% Dark Matter ~25% Dark Energy ~70%
• • • Anti-Matter 0%
10
3. Dark maLer and an@-‐maLer
11
dark maLer
12
solar system
Credit: NASA/JPL
13
solar system
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
13
solar system
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
13
1 v/p r
solar system
Credit: NASA/JPL
Earth revolves around the Sun at 30 km/s
13
a hundred billion stars
28,000 lyrs
Credit: NASA
14 solar system revolves at 220 km/s what is pulling us inside?
a hundred billion stars
28,000 lyrs
Credit: NASA
14 solar system revolves at 220 km/s what is pulling us inside?
a hundred billion stars
28,000 lyrs
Credit: NASA
14 solar system revolves at 220 km/s what is pulling us inside?
a hundred billion stars
28,000 lyrs no stars
Credit: NASA
14
Credit: Jschulman555 hLp://commons.wikimedia.org/wiki/File:NGC_4565_and_4562.jpg
15
Andromeda=2.5M lyrs away also dark maNer important
Credit: NASA
16
Credit: ESA/Hubble and NASA
17
Credit: Vicent Peris, CC BY-‐SA 2.0 hLp://commons.wikimedia.org/wiki/File:NGC_7331_-‐_Peris.jpg
18
Credit: Vicent Peris, CC BY-‐SA 2.0 hLp://commons.wikimedia.org/wiki/File:NGC_7331_-‐_Peris.jpg
18
Vera Rubin 1970’s
Credit: NOAO/AURA/NSF
19
true nature of galaxies 100k lyrs stars
dark maLer
>M lyrs
20
Credit: Based on observa7ons made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collabora7on between the Space Telescope Science Ins7tute (STScI/NASA), the Space Telescope European Coordina7ng Facility (ST-‐ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA), Image processed by c_cld hNp:// www.galaxyzooforum.org/index.php?topic=6927.msg610555#msg610555
21
Credit: Based on observa7ons made with the NASA/ESA Hubble Space Telescope, and obtained from the Hubble Legacy Archive, which is a collabora7on between the Space Telescope Science Ins7tute (STScI/NASA), the Space Telescope European Coordina7ng Facility (ST-‐ECF/ESA) and the Canadian Astronomy Data Centre (CADC/NRC/CSA), Image processed by c_cld hNp:// www.galaxyzooforum.org/index.php?topic=6927.msg610555#msg610555
Cheshire cat
21
cluster of galaxies
Abell 2218 2.1B lyrs Credit: Andrew Fruchter (STScI) et al., WFPC2, HST, NASA
22
Credit: NASA, ESA & L. Calçada
deflec@on angle by a point lens ✓=
4GN m c 2 rc
23
Credit: NASA, ESA & L. Calçada
deflec@on angle by a point lens ✓=
Credit: NASA, Andrew Fruchter and the ERO Team [Sylvia BaggeL (STScI), Richard Hook (ST-‐ECF), Zoltan Levay (STScI)] (STScI)
4GN m c 2 rc
23
Credit: NASA, ESA & L. Calçada
deflec@on angle by a point lens ✓=
Credit: NASA, Andrew Fruchter and the ERO Team [Sylvia BaggeL (STScI), Richard Hook (ST-‐ECF), Zoltan Levay (STScI)] (STScI)
4GN m c 2 rc Credit: J. A. Tyson, UC Davis, LSST
23
image invisible dark maNer
more than 80% of maLer in the Universe is not atoms
24
image invisible dark maNer
more than 80% of maLer in the Universe is not atoms
24
image invisible dark maNer
more than 80% of maLer in the Universe is not atoms
24
4B lyrs away
25
Good not to be here
4B lyrs away
25
Good not to be here
two clusters collided at 4500km/sec 4B lyrs away
25
Good not to be here
two clusters collided at 4500km/sec Credit: J. Wise, M. Bradac (Stanford, KIPAC)
4B lyrs away
25
Good not to be here
two clusters collided at 4500km/sec Credit: J. Wise, M. Bradac (Stanford, KIPAC)
4B lyrs away
25
Good not to be here bullet cluster
two clusters collided at 4500km/sec Credit: J. Wise, M. Bradac (Stanford, KIPAC)
4B lyrs away
25
rs ly 2B
2B lyrs
nearly uniform small wrinkles
rs ly 2B Credit: Sloan Digital Sky Survey
26
10–5 Credit: NASA
we wouldn’t exist without dark maNer
without dark maLer
with dark maLer
27
Reenac@ng the Big Bang with Cal Marching Band
Nobelist George Smoot Directs Big Bang with Cal Band, 12/06 hLp://www.youtube.com/watch?v=OdsWhHWdc1g
28
Reenac@ng the Big Bang with Cal Marching Band
Credit: The Regents of the University of California Nobelist George Smoot Directs Big Bang with Cal Band, 12/06 hLp://www.youtube.com/watch?v=OdsWhHWdc1g
28
OK, I see dark maLer is important. What we do know about it? 29
Cold and Neutral •it must be moving slowly (cold) •it must be electrically neutral •it must be long-lived (at least 13.8Byrs)
30
Dim Stars? Search for MACHOs (Massive Compact Halo Objects) Large Magellanic Cloud
Credit: NASA
31
Dim Stars? Search for MACHOs (Massive Compact Halo Objects) Large Magellanic Cloud Credit: Hubble Heritage Team (AURA/STSCI/NASA)
Credit: NASA
31
Dim Stars? Search for MACHOs (Massive Compact Halo Objects) Large Magellanic Cloud Credit: Hubble Heritage Team (AURA/STSCI/NASA)
Credit: NASA
31
Dim Stars? Search for MACHOs (Massive Compact Halo Objects) Large Magellanic Cloud Credit: Hubble Heritage Team (AURA/STSCI/NASA)
Credit: NASA
Not enough of them!
31
Dim Stars? 0.6
Search for MACHOs (Massive Compact Halo Objects)
EROS collabora@on astro-‐ph/0607207 f = T−7
0.4
Large Magellanic Cloud
MACHO 95% cl EROS−2 + EROS−1 upper limit (95% cl)
0.2
Credit: Hubble Heritage Team 0.0 (AURA/STSCI/NASA) −8 −6 −4 −2
2 0 logM= 2log( t E /70d)
Credit: NASA
Not enough of them!
31
Mass Limits “Uncertainty Principle” •Clumps to form structure •imagine V = G Mrm •“Bohr radius”: r = G M m •too small m ⇒ won’t “fit” in a galaxy! •m >10 eV “uncertainty principle” N
2
B
N
2
−22
bound (modified from Hu, Barkana, Gruzinov, astro-ph/0003365)
32
Summary Mass Limits
Fritz Zwicky Credit: NASA/CXC/ SAO
33
Summary Mass Limits • 10
-31
GeV to 1050 GeV
Fritz Zwicky Credit: NASA/CXC/ SAO
33
Summary Mass Limits • 10 GeV to 10 GeV • narrowed it down to -31
50
within 81 orders of magnitude
Fritz Zwicky Credit: NASA/CXC/ SAO
33
Summary Mass Limits • 10 GeV to 10 GeV • narrowed it down to -31
50
within 81 orders of magnitude
• a big progress in 70 years since Zwicky
Fritz Zwicky Credit: NASA/CXC/ SAO
33
Self-‐Coupling
• if self-coupling too big, will •
“smooth out” cuspy profile at the galactic center some people want it (Spergel and Steinhardt, astro-ph/ 9909386)
• need core < 35 kpc/h from data σ < 1.7 x 10-25 cm2 (m/GeV)
(Yoshida, Springel, White, astro-ph/ 0006134)
• bullet cluster:
σ < 1.7x10-24 cm2 (m/GeV) (Markevitch et al, astro-ph/0309303)
34
•
Self-‐Coupling if self-coupling too big, will “smooth out” cuspy profile at the galactic center
• some people want it
(Spergel and Steinhardt, astro-ph/ 9909386)
• need core < 35 kpc/h from data σ < 1.7 x 10-25 cm2 (m/GeV)
(Yoshida, Springel, White, astro-ph/ 0006134)
• bullet cluster:
σ < 1.7x10-24 cm2 (m/GeV) (Markevitch et al, astro-ph/0309303)
Yoshida et al., 2000
34
MACHO ⇒ WIMP
Credit: NASA
35
MACHO ⇒ WIMP
Credit: NASA
35
MACHO ⇒ WIMP • It is probably WIMP (Weakly Interacting Massive Particle)
• Stable heavy particle produced in early Universe, left-over from near-complete annihilation
• Will focus on WIMPs for the rest or the lecture
Credit: NASA
35 G. Jungman et al. JPhysics Reports 267 (1996) 195-373
221
Using the above relations (H = 1.66g$‘2T 2/mpl and the freezeout condition r = Y~~(G~z~) = H), we find (n&)0 = (n&f
= 1001(m,m~~g~‘2+JA+)
N 10-S/[(m,/GeV)((~A~)/10-27
cm3 s-‘)I,
thermal relic
(3.3)
where the subscript f denotes the value at freezeout and the subscript 0 denotes the value today. The current entropy density is so N 4000 cmm3, and the critical density today is pC II 10-5h2 GeVcmp3, where h is the Hubble constant in units of 100 km s-l Mpc-‘, so the present mass density in units of the critical density is given by 0,h2 = mxn,/p, N (3 x 1O-27 cm3 C1/(oAv))
• • • • • •
.
(3.4)
The result is independent of the mass of the WIMP (except for logarithmic corrections), and is inversely proportional to its annihilation cross section. Fig. 4 shows numerical solutions to the Boltzmann equation. The equilibrium (solid line) and actual (dashed lines) abundances per comoving volume are plotted as a function of x = m,/T
thermal equilibrium when kT>mχc2 Once kT<mχc2, no more χ created if stable, only way to lose them is annihilation but universe expands and χ get dilute at some point they can’t find each other their number in comoving volume “frozen”
0 . 01 0 . 001
0 . 0001 10-b
10-s
,h -;
10-7
caJ 10-a
a
10-Q
2 p
lo-‘9
$
lo-”
z
10-m
F!
lo-‘3
10
x=m/T
100
(time
Fig. 4. Comoving number density of a WIMP in the early Universe. the solid curve is the equilibrium abundance. From [31].
+) The dashed
curves are the actual abundance,
and
36
Order of magnitude • “Known” Ω =0.23 χ
determines the WIMP annihilation cross section
• simple estimate of
⇤ g⇥
⌅⇤ann v⇧ ⇤
the annihilation cross ⇥ 10 section
• within the range at LHC!!!
1/2
xf s0 MP3 l ⌅⇤ann v⇧ H02
1.12
GeV 2 ⇥ 2 ⌅⇤ann v⇧ ⇤ 2 m m ⇤ 300 GeV 9
10
10
GeV
1/2 g⇥
2
xf
h2
37
Listen to faint sound can’t hear faint sound
38
Listen to faint sound can’t hear faint sound
shut out the noise!
38
Listen to faint sound can’t hear faint sound
shut out the noise!
to hear faint sound of dark maLer ???? go to quiet space＝underground
38
Listen to faint sound can’t hear faint sound
shut out the noise!
to hear faint sound of dark maLer go to quiet space＝underground
38
39
basic idea • maximum energy
nucleus
transfer to nucleus when mχ~MA
DM
nucleus
• energy of the nucleus leads to a combination of
• ionization • phonon • scintillation
DM
Ef =
1 m MA m v2 2(1 2 (m + MA )2
ˆ cos ✓)
40 December 24, 2009
2010 Jan 21
Y. Suzuki (IPMU Site Visit) @Kashiwa
25
41
XMASS 1t liquid Xenon in Kamioka mine
42 Rene Ong
WIMP Direct Detection Limits Spin Independent
Spin Dependent
potential signals
COUPP Xenon100
Super K Super-K
MSSM
IceCube
MSSM
(Potential signals: DAMA/LIBRA, CRESST, CoGeNT – see backup slides)
43 Rene Ong
WIMP Direct Detection Limits
Exci7ng! Spin Independent
Spin Dependent
potential signals
COUPP Xenon100
Super K Super-K
MSSM
IceCube
MSSM
(Potential signals: DAMA/LIBRA, CRESST, CoGeNT – see backup slides)
43
LHC E=mc2 Credit: CERN, Photograph: Maximilien Brice
Can we make dark maNer? Credit: CERN
44
• Something is escaping the detector ⇒Dark Matter!?
| 500cm
0
energy and momenta are unbalanced “missing energy” Emiss
Y
• Mimic Big Bang in the lab • Hope to create invisible Dark Matter particles • Look for events where
4.8Gev EC 19.Gev HC
500cm|
Producing Dark MaLer in the laboratory
| 500cm YX hist.of BA.+E.C.
0
X
500cm|
Credit: CERN
45
program
cosmic abundance
of dark matter • cosmological measurement −1 abundance ∝ σ • ann • detection experiments • scattering cross section • production at colliders • mass, couplings • can calculate cross sections • If they agree with each other:
⇒ ⇒
LHC
WMAP
Will know what Dark MaHer is Will understand universe back to t∼10-10 sec
ILC
mass of the Dark Matter
46
yrs
yrs
8B
0k
t ion rill
in
13.
38
3m
1t ec hs
CMB
Higgs
Credit: C. Amsler et al. (Par@cle Data Group), Physics LeLers B667, 1 (2008)
47
yrs
yrs
8B
0k
in
13.
38
3m
sec nth llio -bi ten sec th ion rill
1t
Higgs DM
CMB
Credit: C. Amsler et al. (Par@cle Data Group), Physics LeLers B667, 1 (2008)
47
Neutrinos and an@-‐maLer
48
Credit: NASA
49
Credit: NASA
49
An@-‐MaLer •for every particle, there is an antiparticle
•same mass, same lifetime •opposite electric charge •electron e and positron e_ •proton p and anti-proton p _ •neutron n and anti-neutron n –
+
50
51
1933 first humanmade an@-‐maLer
51
γ photon 1933 first humanmade an@-‐maLer
51
e− electron
γ photon 1933 first humanmade an@-‐maLer
51
e− electron
e+ positron
γ photon 1933 first humanmade an@-‐maLer
51
e− electron
Irène
e+ positron
γ photon Frédéric Joliot-‐Curie
1933 first humanmade an@-‐maLer
51
Berkeley
Credit: © 2010 The Regents of the University of California, Lawrence Berkeley Na@onal Laboratory
52
Berkeley
1955 an@-‐proton
maLer and an@-‐ maLer annihilate into pure energy Credit: © 2010 The Regents of the University of California, Lawrence Berkeley Na@onal Laboratory
52
Berkeley
1955 an@-‐proton
Emilio Owen Segrè Chamberlain maLer and an@-‐ maLer annihilate into pure energy Credit: © 2010 The Regents of the University of California, Lawrence Berkeley Na@onal Laboratory
Credit: CERN
\CM : $ &#IMP
8
CM\
'EV%# 'EV(#
Q
52
53
98HISTOF"! %# \CM
9
CM\
an@-‐maLer at use
Positron Emission Tomography (PET)
Typical PET Facility
54
Credit: NIDA, NIH
55
56
Credit: Positronics Research, LLC
56
Credit: Positronics Research, LLC
E=mc2 300 million @mes more efficient than regular gasoline
56
Energy sources •eV=1.6×10 J •for each proton m c =0.938GeV •chemical reaction ~eV •nuclear fission ~MeV •nuclear fusion ~10MeV •anti-matter (proton on anti-proton) –19
p
2
~GeV
57
58
• European Laboratory CERN
• A scientist produced
a quarter gram of anti-matter without the knowledge of the Director General
• falls into wrong hands!
58
• European Laboratory CERN
• A scientist produced
a quarter gram of anti-matter without the knowledge of the Director General
• falls into wrong hands!
billion trillion trillion dollars
58
• European Laboratory CERN
• A scientist produced
a quarter gram of anti-matter without the knowledge of the Director General
• falls into wrong hands!
billion trillion trillion dollars
58
Early Universe 1,000,000,002
1,000,000,000
matter
anti-matter 59
Current Universe 2 us
anti-matter
matter
We won! But why?
60
Beginning of Universe 1,000,000,001
1,000,000,001
anti-matter
matter
61
frac@on of second later 1 1,000,000,002
matter
1,000,000,000
anti-matter
turned a billionth of an@-‐maLer to maLer
62
Universe Now 2 us
matter
anti-matter
This must be how we survived the Big Bang!
63
Life or Death
64
Life or Death • Is the world of anti-matter the exact mirror of the world of matter?
64
Life or Death • Is the world of anti-matter the exact mirror of the world of matter? • If so, there is no reason for matter to be chosen
64
Life or Death • Is the world of anti-matter the exact mirror of the world of matter? • If so, there is no reason for matter to be chosen • It shouldn’t be an exact mirror. There must be some subtle difference!
64
Life or Death • Is the world of anti-matter the exact mirror of the world of matter? • If so, there is no reason for matter to be chosen • It shouldn’t be an exact mirror. There must be some subtle difference! • How can such a difference be explained? 64
Life or Death • Is the world of anti-matter the exact mirror of the world of matter? • If so, there is no reason for matter to be chosen • It shouldn’t be an exact mirror. There must be some subtle difference! • How can such a difference be explained? • A bold 1973 theory by Kobayashi and Maskawa (2008 Nobel prize in physics)
64
Elementary Par@cles Credit: Marekich, CC BY-‐SA 3.0
nuclei
atoms
protons
neutrons
quarks
Credit: NASA
65
Elementary Par@cles Credit: Marekich, CC BY-‐SA 3.0
nuclei
atoms
protons
neutrons
quarks down
Credit: NASA
up
65
Elementary Par@cles Credit: Marekich, CC BY-‐SA 3.0
nuclei
atoms
protons
neutrons
quarks down
Credit: NASA
electron
down
up
up
65
Elementary Par@cles Credit: Marekich, CC BY-‐SA 3.0
nuclei
atoms
protons
neutrons
quarks down
Credit: NASA
muon
electron
down
up
up
65
Elementary Par@cles Credit: Marekich, CC BY-‐SA 3.0
nuclei
atoms
protons Who ordered that?? muon I.I. Rabi electron down
neutrons
quarks down
Credit: NASA
up
up
65
Muons
66
Muons
Muons come from outer space. About a thousand of them go through our body every minute like X-‐ray.
66 Science 167, 832 (1970)
Credit: Ricardo Liberato, CC BY-‐SA 3.0
Search for Hidden Chambers in the Pyramids The structure of the Second Pyramid of Giza is determined by cosmic-ray absorption Luis W. Alvarez, Jared A. Anderson, F. El Bedwei, James Burkhard, Ahmed Fakhry, Adib Girgis, Amr Goneid, Fikhry Hassan, Dennis Iverson, Gerald Lynch, Zenab Miligy, Ali Hilmy Moussa, Mohammed Sharkawi, Lauren Yazolino
67 Science 167, 832 (1970)
Credit: Ricardo Liberato, CC BY-‐SA 3.0
Search for Hidden Chambers in the Pyramids The structure of the Second Pyramid of Giza is determined by cosmic-ray absorption Luis W. Alvarez, Jared A. Anderson, F. El Bedwei, James Burkhard, Ahmed Fakhry, Adib Girgis, Amr Goneid, Fikhry Hassan, Dennis Iverson, Gerald Lynch, Zenab Miligy, Ali Hilmy Moussa, Mohammed Sharkawi, Lauren Yazolino
67
Credit: Ricardo Liberato, CC BY-‐SA 3.0
Science 167, 832 (1970) Search for Hidden Chambers in the Pyramids The structure of the Second Pyramid of Giza is determined by cosmic-ray absorption Luis W. Alvarez, Jared A. Anderson, F. El Bedwei, James Burkhard, Ahmed Fakhry, Adib Girgis, Amr Goneid, Fikhry Hassan, Dennis Iverson, Gerald Lynch, Zenab Miligy, Ali Hilmy Moussa, Mohammed Sharkawi, Lauren Yazolino
hidden chamber with treasures?
67 Credit: Ricardo Liberato, CC BY-‐SA 3.0
Science 167, 832 (1970) Search for Hidden Chambers in the Pyramids The structure of the Second Pyramid of Giza is determined by cosmic-ray absorption Luis W. Alvarez, Jared A. Anderson, F. El Bedwei, James Burkhard, Ahmed Fakhry, Adib Girgis, Amr Goneid, Fikhry Hassan, Dennis Iverson, Gerald Lynch, Zenab Miligy, Ali Hilmy Moussa, Mohammed Sharkawi, Lauren Yazolino
hidden chamber with treasures?
67 Credit: Ricardo Liberato, CC BY-‐SA 3.0
Science 167, 832 (1970) Search for Hidden Chambers in the Pyramids The structure of the Second Pyramid of Giza is determined by cosmic-ray absorption Luis W. Alvarez, Jared A. Anderson, F. El Bedwei, James Burkhard, Ahmed Fakhry, Adib Girgis, Amr Goneid, Fikhry Hassan, Dennis Iverson, Gerald Lynch, Zenab Miligy, Ali Hilmy Moussa, Mohammed Sharkawi, Lauren Yazolino
hidden chamber with treasures?
No hidden chamber!
•
67
see through a volcano use cosmic ray muons to see the inside of a volcano
•can locate magma •demonstrated by
Earthquake Research Institute, Univ. of Tokyo
•useful for
predicting eruption
Credit: © Center for High Energy Geophysics Research, Earthquake Research Ins@tute, University of Tokyo
68
•
see through a volcano use cosmic ray muons to see the inside of a volcano
•can locate magma •demonstrated by
Earthquake Research Institute, Univ. of Tokyo
•useful for
predicting eruption
Credit: © Center for High Energy Geophysics Research, Earthquake Research Ins@tute, University of Tokyo
68
69 Luis Walter Alvarez
69
Elementary Par@cles
muon electron
down
up
70
Elementary Par@cles
muon
strange
electron
down
up
70
Elementary Par@cles
Credit: NIMSoffice, CC BY-‐SA 3.0
There must be three of each type muon
strange
electron
down
up
70
Elementary Par@cles
Credit: NIMSoffice, CC BY-‐SA 3.0
There must be three of each type muon
strange
electron
down
charm
1974
up
70
Elementary Par@cles
Credit: NIMSoffice, CC BY-‐SA 3.0
There must be tau of e1975 three ach type muon electron
strange down
charm
1974
up
70
Elementary Par@cles
Credit: NIMSoffice, CC BY-‐SA 3.0
There must be bottom tau of e1975 three ach type muon
1978
strange
electron
charm
down
1974
up
70
Elementary Par@cles top
1995
Credit: NIMSoffice, CC BY-‐SA 3.0
There must be bottom tau of e1975 three ach type muon electron
strange down
1978
charm
1974
up
70
Why three?
71
Why three? • essential difference
between two and three
71
Why three? • essential difference between two and three • connect the dots
71
Why three? • essential difference between two and three • connect the dots
71
Why three? • essential difference between two and three • connect the dots
71
Why three? • essential difference between two and three • connect the dots
71
Why three? • essential difference between two and three • connect the dots
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter
correspond to reflection
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter
correspond to reflection
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter correspond to reflection • can make a difference!
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter correspond to reflection • can make a difference!
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter correspond to reflection • can make a difference!
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter correspond to reflection • can make a difference!
71
Why three? • essential difference between two and three • connect the dots • three or more leads to polygons • matter and anti-matter correspond to reflection • can make a difference! • but with two dots, a polygon collapses
71
Major experiments
Credit: SLAC Na@onal Accelerator Laboratory
72
Major experiments
•Head-to-head competition between
Stanford/Berkeley and KEK (Japan)
Credit: SLAC Na@onal Accelerator Laboratory
72
Major experiments
•Head-to-head competition between
Stanford/Berkeley and KEK (Japan)
•
Credit: SLAC Na@onal Accelerator Laboratory
Super high-tech machine with micron precision over 4 miles and colliding beams every 4 nanoseconds at speed of light
72
Credit: © 2009 The Regents of the University of California
73
Credit: © 2009 The Regents of the University of California
73
Difference between maLer and an@-‐maLer
74
Difference between maLer and an@-‐maLer
• Three found as they predicted
74
Difference between maLer and an@-‐maLer
• Three found as they predicted
• Then there must be
some difference between matter and anti-matter!
74
Difference between maLer and an@-‐maLer
• Three found as they predicted
• Then there must be
some difference between matter and anti-matter!
• Experiments at
Stanford and KEK confirmed their prediction precisely since 2002
74
• Three found as they predicted
• Then there must be
some difference between matter and anti-matter!
• Experiments at
Stanford and KEK confirmed their prediction precisely since 2002
Asymmetry Entries / 0.5 ps
Difference between maLer and an@-‐maLer
Belle
0
0
400 (d) B m J/YK 300 200 B0 100 0
_ B0
q=+1 q= 1
0.5 0
-0.5 -7.5 -5 -2.5
0
2.5
-X f $t(ps)
5
7.5
74
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
75
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
•We could explain the subtle difference
between matter and anti-matter thanks to Kobayashi and Maskawa
75
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
•We could explain the subtle difference •
between matter and anti-matter thanks to Kobayashi and Maskawa Can we then explain the difference of one part in billion in our Universe?
75
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
•We could explain the subtle difference • •
between matter and anti-matter thanks to Kobayashi and Maskawa Can we then explain the difference of one part in billion in our Universe? We can only explain 10–26!
75
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
•We could explain the subtle difference • • •
between matter and anti-matter thanks to Kobayashi and Maskawa Can we then explain the difference of one part in billion in our Universe? We can only explain 10–26! more differences are needed
75
New Puzzle Credit: NIMSoffice, CC BY-‐SA 3.0
•We could explain the subtle difference • • • •
between matter and anti-matter thanks to Kobayashi and Maskawa Can we then explain the difference of one part in billion in our Universe? We can only explain 10–26! more differences are needed we also need to see how anti-matter can turn into matter
75
New Paradigm •Maybe neutrinos could reshuffle the
balance between matter and anti-matter
•Possible if neutrino can morph into antineutrino and back
•Then we owe our existence to neutrinos!
76
New Paradigm •Maybe neutrinos could reshuffle the
balance between matter and anti-matter
•Possible if neutrino can morph into antineutrino and back
•Then we owe our existence to neutrinos! Fukugita Yanagida
76
Neutrinos morph KamLAND
1kt
uses mineral oil (liquid scin@llator) instead of water
Credit: KamLAND collabora@on
77
78
• • •
Credit: KamLAND collabora@on
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2
Survival Probability
Neutrinos morph There are three types of neutrinos (electron, muon, tau) one species changes into another neutrinos oscillate
1 0.8 ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.6 0.4 0.2 0 10
-3
10
-2
10
-1
10
1
20
30
40
50
60
70
80
L 0/E (km/MeV)
79
Neutrinos morph
• There are three types of neutrinos (electron, muon, tau) • one species changes into another • neutrinos oscillate
1 0.8 ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.6 0.4
0 10
-3
10
-2
10
h
0.2
p mor
Survival Probability
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2
Credit: KamLAND collabora@on
-1
10
1
20
30
40
50
60
70
80
L 0/E (km/MeV)
79
Neutrinos morph
• There are three types of neutrinos (electron, muon, tau) • one species changes into another • neutrinos oscillate
1 0.8
0.2 0 10
-3
10
-2
10
-1
ba ck
0.4
h
ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.6
p mor
Survival Probability
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2
Credit: KamLAND collabora@on
1
10
20
30
40
50
60
70
80
L 0/E (km/MeV)
79
Neutrinos morph
• There are three types of neutrinos (electron, muon, tau) • one species changes into another • neutrinos oscillate
1 0.8 ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.4
0 10
-3
10
-2
10
h
0.2
m or ph
ba ck
0.6
p mor
Survival Probability
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2
Credit: KamLAND collabora@on
-1
10
1
20
30
40
50
60
70
80
L 0/E (km/MeV)
79
• • •
Credit: KamLAND collabora@on
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2 1
0 10
-3
10
-2
10
ck
h
0.2
m or ph
ba
0.4
-1
10
1
20
30
40
ba
ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.6
ck
0.8
p mor
Survival Probability
Neutrinos morph There are three types of neutrinos (electron, muon, tau) one species changes into another neutrinos oscillate
50
60
70
80
L 0/E (km/MeV)
79
Neutrinos morph
• There are three types of neutrinos (electron, muon, tau) • one species changes into another • neutrinos oscillate
1
0.2 0 10
-3
10
-2
10
-1
m or ph
ba ck
0.4
h
ILL Goesgen Savannah River Palo Verde CHOOZ Bugey Rovno Krasnoyarsk
0.6
1
10
20
30
40
ba ck
0.8
p mor
Survival Probability
KamLAND data Neutrino oscillation with real reactor distribution
previous reactor experiments
1.2
Credit: KamLAND collabora@on
50
60
70
80
L 0/E (km/MeV)
79
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
80
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
80
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
80
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
80
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
80
Turn an@-‐maLer into maLer
• Can anti-matter turn into matter?
• Maybe anti-neutrino can
turn into neutrino because they don’t carry electricity
• 0νββ: nn→ppe–e– with no neutrinos
• can happen only once 10
24
(trillion trillion) years
paLence!
80
Need big underground experiments • look for 136 Xe ! 136 Ba e • dissolve gaseous xenon
e
into liquid scintillator
• current 100kg of enriched xenon
• so far only upper25limit
⌧1/2 > 3.4 ⇥ 10 years
KamLAND=1000t
Credit: KamLAND collabora@on
81
Need big underground experiments • look for 136 Xe ! 136 Ba e • dissolve gaseous xenon
e
into liquid scintillator
• current 100kg of enriched xenon
• so far only upper25limit
⌧1/2 > 3.4 ⇥ 10 years
KamLAND=1000t
Credit: KamLAND collabora@on
81
look for difference _ between ν and ν T2K
compare P (⌫µ ! ⌫e ) and P (¯⌫µ ! ⌫¯e )
82
1300km!
83
yrs
rs
ky
8B
13.
380
in 3m
ec th s lion -bil sec ten nth illio
1 tr
Higgs
CMB
DM
Credit: C. Amsler et al. (Par@cle Data Group), Physics LeLers B667, 1 (2008)
84
8B
13. yrs
rs
ky
DM
380
10
in 3m
ec th s lion -bil sec ten nth illio nds eco -26 s 1 tr
Higgs an7-‐maNer!
CMB
Credit: C. Amsler et al. (Par@cle Data Group), Physics LeLers B667, 1 (2008)
84
